The small scale environment of low surface brightness disk galaxies

Bothun, G. D.; Schombert, James M.; Impey, C.; Sprayberry, David; McGaugh, Stacy S.

doi:10.1086/116659

Cited by 95 publications

(112 citation statements)

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“…Other authors probed the environment of LSBs on intermediate and small scales. It was found that on scales below 2 Mpc, the galaxy environment of LSBs is less dense than that of HSBs (Bothun et al 1993;Mo et al 1994). Furthermore, a lack of nearby (r ≤ 0.5 Mpc) companions of LSB galaxies was detected by Zaritsky & Lorrimer (1993).…”

Section: Discussionmentioning

confidence: 99%

The large-scale environment of low surface brightness galaxies

Rosenbaum

Krusch

Bomans

et al. 2009

A&A

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Context. The exact formation scenarios and evolutionary processes that led to the existence of the class of low surface brightness galaxies (LSBs) have not yet been understood completely. There is evidence that the lack of star formation expected to be typical of LSBs can only occur if the LSBs were formed in low-density regions. Aims. Since the environment of LSBs has been studied before only on small scales (below 2 Mpc), a study of the galaxy content in the vicinity of LSB galaxies on larger scales could add a lot to our understanding of the origin of this galaxy class. Methods. We used the spectroscopic main galaxy sample of the SDSS DR4 to investigate the environmental galaxy density of LSB galaxies compared to the galaxy density in the vicinity of high surface brightness galaxies (HSBs). To avoid the influence of evolutionary effects depending of redshift and to minimize completeness issues within the SDSS, we limited the environment studies to the local universe with a redshift of z ≤ 0.1. At first we studied the luminosity distribution of the LSB sample obtained from the SDSS within two symmetric redshift intervals (0.01 < z ≤ 0.055 and 0.055 < z ≤ 0.1). Results. It was found that the lower redshift interval is dominated by small, low-luminosity LSBs, whereas the LSB sample in the higher redshift range mainly consists of larger, more luminous LSBs. This comes from selection effects of the SDSS spectroscopic sample. The environment studies, also divided into these two redshift bins, show that both the low mass, and the more massive LSBs possess an environment with a lower galaxy density than HSBs. The differences in the galaxy density between LSBs and HSBs are significant on scales between 2 and 5 Mpc, the scales of groups and filaments. To quantify this, we have introduced for the first time the LSB-HSB Antibias. The obtained LSB-HSB Antibias parameter has a value of 10%-15%. Conclusions. From these results we conclude that LSBs formed in low-density regions of the initial universe and have drifted until now to the outer parts of the filaments and walls of the large-scale structure. Furthermore, our results, together with actual cosmological simulations, show that LSBs are caused by a mixture of nature and nurture.

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Section: Discussionmentioning

confidence: 99%

The large-scale environment of low surface brightness galaxies

Rosenbaum

Krusch

Bomans

et al. 2009

A&A

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“…1989 ;Salzer et al 1990 ;Bothun et al 1993 ;Pustilnik et al 1995 ;Lindner et al 1996 ;Lee et al 2000). In some cases the nearest reference ordinary galaxy is about equally close to test and ordinary galaxies.…”

Section: Nearest Neighbor Statisticsmentioning

confidence: 97%

“…(1989), Binggeli, Tarenghi, & Sandage (1990), Bothun et al (1993), Lindner et al (1996), Kuhn, Hopp, & Elsasser (1997), Schombert, Pildis, & Eder (1997), Popescu, Hopp, & (1997), Lee et al (2000), and El-Ad & Piran (2000).…”

Section: Oidsmentioning

confidence: 98%

The Void Phenomenon

Peebles

2001

ApJ

315

362

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Advances in theoretical ideas on how galaxies formed have not been strongly inÑuenced by the advances in observations of what might be in the voids between the concentrations of ordinary optically selected galaxies. The theory and observations are maturing, and the search for a reconciliation o †ers a promising opportunity to improve our understanding of cosmic evolution. I comment on the development of this situation and present an update of a nearest neighbor measure of the void phenomenon that may be of use in evaluating theories of galaxy formation.

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“…Bothun et al 1986aBothun et al , 1993Mo et al 1994), in the sense that they tend to avoid clusters, and are not found close to field galaxies. However, this is based on comparison with galaxy catalogues that are badly incomplete for dwarf galaxies, and especially for LSBGs and dEs.…”

Section: The Spatial Distribution Of Metal-poor Galaxiesmentioning

confidence: 99%

The most metal-poor galaxies

Kunth

Östlin

2000

Astronomy and Astrophysics Review

375

428

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Metallicity is a key parameter that controls many aspects in the formation and evolution of stars and galaxies. In this review we focus on the metal deficient galaxies, in particular the most metal-poor ones, because they play a crucial rôle in the cosmic scenery. We first set the stage by discussing the difficult problem of defining a global metallicity and how this quantity can be measured for a given galaxy. The mechanisms that control the metallicity in a galaxy are reviewed in detail and involve many aspects of modern astrophysics: galaxy formation and evolution, massive star formation, stellar winds, chemical yields, outflows and inflows etc. Because metallicity roughly scales as the galactic mass, it is among the dwarfs that the most metalpoor galaxies are found. The core of our paper reviews the considerable progress made in our understanding of the properties and the physical processes that are at work in these objects. The question on how they are related and may evolve from one class of objects to another is discussed. While discussing metal-poor galaxies in general, we present a more detailed discussion of a few very metal-poor blue compact dwarf galaxies like IZw18. Although most of what is known relates to our local universe, we show that it pertains to our quest for primeval galaxies and is connected to the question of the origin of structure in the universe. We discuss what QSO absorption lines and known distant galaxies tell us already? We illustrate the importance of star-forming metal-poor galaxies for the determination of the primordial helium abundance, their use as distance indicator and discuss the possibility to detect nearly metal-free galaxies at high redshift from Lyα emission.

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The small scale environment of low surface brightness disk galaxies

Cited by 95 publications

References 1 publication

The large-scale environment of low surface brightness galaxies

The large-scale environment of low surface brightness galaxies

The Void Phenomenon

The most metal-poor galaxies

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